Stein (1996) only identifies the galaxies by his own sequential ID numbers
and the position
.
Cross-identification with the Richter (1989) `R' ID numbers
for the 70 galaxies selected as described above
was made by forming all possible (Stein,Richter) galaxy pairs.
For each pair the coordinate distance between the two galaxies in the pair was
computed, and the pairs were then sorted after coordinate distance.
37 pairs had a distance of less than 4''.
The following pairs had distances of 5.3'', 6.0'', 13.3'', and
24.5''. The first 3 were clear matches, since the heliocentric velocity
from Stein
differed by at most 2% from that of Richter.
The fourth was a clear mismatch, since that Stein ID had already been
matched to a Richter ID further up the list.
Thus 40 galaxies from the Stein catalog were also in
the above subset of the Richter catalog.
The established cross-identification for these 40 galaxies can be seen
in Table

Poulain & Nieto (1994) write:
``Foreground stars, when visible through the eye-piece,
were measured through the smallest aperture available
(10.9 arcsec [in diameter /BMJ]) and their contribution subtracted
at a later stage.''
In their Table 1a, they note whether the given galaxy had
one or more stars subtracted.
The two galaxies in common with our study had no stars subtracted.

Burstein et al. (1987) write:
``Separate observations of contaminating stars are noted
[in their Table 2 /BMJ] by asterisks in the columns headed by ``Run''
and ``N'' (notes); star observations always refer to the immediately
preceding galaxy observation.''
One of the four galaxies in common with our study, R256,
had one star subtracted.

Sandage (1975) writes:
``Contaminating stars were were present in some of the apertures
as notes in Table 1. Measurements of the stars alone, using smaller
apertures, are listed where appropriate. Contamination-free colors and
magnitudes were calculated for the final reduction.''
One of the two galaxies in common with our study, R256,
had one star subtracted.

To get a rest frame wavelength interval that is
common to the galaxy and the star,
their relative radial velocity needs to be known.
The program uses the input guess on the radial velocity
to do this.
We computed an accurate such input guess
by cross-correlating the two spectra using the task
stsdas.contrib.xcor.

A common galaxy/star rest frame wavelength interval of the same length
was used for all the galaxies.
It was defined by always skipping the 130 most blue columns in
the galaxy spectrum,
and then skipping the number of columns in the template star spectrum
required to shift it onto the galaxy spectrum rest frame wise.
This latter number depends on the redshift of the galaxy.
830 columns were used for the fitting, skipping 64 columns in the red end
of the spectrum to stay clear of the position of the very strong
5577 Å sky line.
The resulting wavelength interval was of length 534 Å.

This corresponds to the line
,
which is what is shown in Fig. 2b in Bender et al. (1992).
These authors define a new 3-space
in which
the
projection shows the FP nearly face-on.
Note, that in the text of Bender et al.,
the line is given as
,
a line that fall just inside the the distribution of galaxies,
not at the edge.
The relation
is also what is used recently by
Burstein et al. (1997).

No overlap photometry on stars using phot
was done involving field 24, but for the galaxy R243
located in the overlap between
field 24 night 4 and field 23 night 3,
an offset
is available.
At the 10.08'' aperture, it is
in GR and
in JB.

To these
magnitude differences at a finite aperture r,
,
should be added the difference in
aperture correction induced by the difference in seeing,
,
to get the intrinsic
magnitude difference,
;
i.e.
.
for those
particular images and the used 9 pixel aperture is
-0.002 for GR and -0.003 for JB, and thus negligible.
For reference,
the seeing values are listed in
Table
(p. ),
the aperture correction vs. seeing is plotted in
Fig. (p. ) and
(p. ),
and the pixel scale is 0.5073 ''/pixel.

It should be noted, that the output
from the mknobsfile in digiphotx.photcalx and
from the mknobsfile in digiphot.photcal
is not in the same format:
the x version has eight columns with OTIME as the third,
the non-x version has only seven columns, and does not have OTIME.
Here, the x version was used.